Time-Distance Helioseismic Image of Solar Tachocline Area

Details Time-Distance Helioseismic Image of Solar Tachocline Area Time-Distance Helioseismic Image of Solar Tachocline Area

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp21a..02z&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP21A-02

Computer Science

Sound

7522 Helioseismology

Scientific paper

Solar tachocline is an area located at the bottom of solar convection zone. It is also a location where sound speed exhibits a bump relative to the standard solar model, and where solar rotation has a large shear. Tachocline is generally believed as the location where solar dynamo operates, therefore, it is important and interesting to image its structure, as well as its structure evolution with solar cycle. Using both surface- and deep-focusing time-distance helioseismology techniques, we have designed measurement schemes and developed inversion codes to derive sound speed perturbations at the tachocline area. Those codes are tested on numerically simulated data, which simulates the global acoustic wavefields with an artificial tachocline model. After getting some satisfactory results from simulation data, we apply the technique on SOHO/MDI medium-l data, and study the acoustic structure of solar interior, as well as its evolution with the solar cycle.

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